Search results for "Pulsar planet"

showing 4 items of 4 documents

SAX J1808.4-3658, an accreting millisecond pulsar shining in gamma rays?

2016

We report the detection of a possible gamma-ray counterpart of the accreting millisecond pulsar SAX J1808.4-3658. The analysis of ~6 years of data from the Large Area Telescope on board the Fermi Gamma-ray Space Telescope (Fermi-LAT) within a region of 15deg radius around the position of the pulsar reveals a point gamma-ray source detected at a significance of ~6 sigma (Test Statistic TS = 32), with position compatible with that of SAX J1808.4-3658 within 95% Confidence Level. The energy flux in the energy range between 0.6 GeV and 10 GeV amounts to (2.1 +- 0.5) x 10-12 erg cm-2 s-1 and the spectrum is well-represented by a power-law function with photon index 2.1 +- 0.1. We searched for si…

Astrophysics::High Energy Astrophysical PhenomenaPulsar planetEnergy fluxFOS: Physical sciencesGamma-rays: starAstrophysics01 natural sciencesBinary pulsarSettore FIS/05 - Astronomia E AstrofisicaSpitzer Space TelescopePulsarMillisecond pulsar0103 physical sciences010303 astronomy & astrophysicsPhysicsHigh Energy Astrophysical Phenomena (astro-ph.HE)010308 nuclear & particles physicsAstronomyAstronomy and AstrophysicsStars: neutronStars: individual: SAX J1808.4-3658Space and Planetary ScienceOrbital motionstars; Stars: individual: SAX J1808.4-3658; Stars: neutron; Space and Planetary Science; Astronomy and Astrophysics [Gamma-rays]Astrophysics - High Energy Astrophysical PhenomenaFermi Gamma-ray Space Telescope
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PSR J1012+5307: younger than it looks?

1998

Lorimer et al. have recently reported that the spin-down age (∼7 × 109 yr) of the low-mass binary pulsar PSR J1012+5307 is much higher than the cooling age (3 × 108 yr) of its white dwarf companion. The proposed solutions for this discrepancy are outlined and discussed. In particular, the revised cooling age estimate proposed by Alberts et al. agrees with data from other low-mass binary pulsar systems if a transition to the ‘classical’ cooling regime occurs between ∼0.14 and ∼0.28 M⊙. If this transition is excluded, PSR J1012+5307 seems to have finished its accretion phase far from the spin-up line.

PhysicsAccretion (meteorology)Astrophysics::High Energy Astrophysical PhenomenaPulsar planetAstronomyWhite dwarfAstronomy and AstrophysicsAstrophysicsBinary pulsarNeutron starPulsarSpace and Planetary ScienceMillisecond pulsarAstrophysics::Galaxy AstrophysicsLine (formation)Monthly Notices of the Royal Astronomical Society
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PSR 1758 – 24 and G5.4 – 1.2, a remarkable pulsar–supernova remnant association

1991

Τiming observations made over an 18-month period using the Parkes radiotelescope show that the pulsar PSR 1758-24 is young and is located at the extreme western edge of the compact nebula G5.27-0.90 which is associated with supernova remnant G5.4-1.2. These results confirm the association of this pulsar with the supernova remnant. They also imply that the pulsar was born with such a high velocity that is has overtaken the supernova remnant shell and now lies outside the shell

PhysicsNebulaAstrophysics::High Energy Astrophysical PhenomenaPulsar planetAstrophysics::Instrumentation and Methods for AstrophysicsAstronomyAstronomy and AstrophysicsAstrophysicsRadio telescopeNeutron starPulsarSpace and Planetary ScienceMillisecond pulsarAstrophysics::Solar and Stellar AstrophysicsSupernova remnantStellar evolutionAstrophysics::Galaxy AstrophysicsMonthly Notices of the Royal Astronomical Society
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The age of PSR J1012 + 5307

1996

PhysicsSpace and Planetary ScienceMillisecond pulsarPulsar planetAstronomy and AstrophysicsMonthly Notices of the Royal Astronomical Society
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